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Low-resolution spectra from 3000-9000 AA of young low-mass stars and browndwarfs were obtained with LRIS on Keck I. The excess UV and optical emissionarising in the Balmer and Paschen continua yields mass accretion rates rangingfrom 2e-12 to 1e-8 Mo/yr. These results are compared with {\it HST}/STISspectra of roughly solar-mass accretors with accretion rates that range from2e-10 to 5e-8 Mo/yr. The weak photospheric emission from M-dwarfs at <4000 Aleads to a higher contrast between the accretion and photospheric emissionrelative to higher-mass counterparts. The mass accretion rates measured hereare systematically 4-7 times larger than those from H-alpha emission lineprofiles, with a difference that is consistent with but unlikely to beexplained by the uncertainty in both methods. The accretion luminositycorrelates well with many line luminosities, including high Balmer and many HeI lines. Correlations of the accretion rate with H-alpha 10% width and linefluxes show a large amount of scatter. Our results and previous accretion ratemeasurements suggest that accretion rate is proportional to M^(1.87+/-0.26) foraccretors in the Taurus Molecular Cloud.

UV excess measures of accretion onto young very low-mass stars and brown dwarfs